themis/artemis, fall swt 1 sep. 14-16, 2011 artemis themis mission accomplishments, status li et al....

THEMIS/ARTEMIS, Fall SWT 1 Sep. 14-16, 2011

ARTEMIS

THEMISMission accomplishments, status

Li et al. 2009GRL Cover

Bortnik et al.2008 Science

JGR special isssue on Substorms , 2011

GRL,Special Issue, 2008

Special Issue, 2008

PRL cover, 2009

TH-ATH/GBO

Nishimura et al.2010, Science

Halekas et al. 2010, SSRTao et al., 2011, JGR

Wiehle et al. 2011, JGR

AGU Geophys..Monogr. Ser. , 2012

THEMIS

ARTEMIS



ARTEMIS

THEMIS

Output• Number of publications per year steadily increasing

Source: http://themis.ssl.berkeley.edu/publications.shtml


ARTEMIS

THEMIS

Programmatics• Since Senior Review 2010:

THEMIS/ARTEMIS extended through 2014 Planetary Division has also endorsed ARTEMIS (w/ minimal funding) No new/revised contract with GSFC to account for the Science uptick Visiting scholars program in place (Quanqi Shi, Robert Michell, Marilia Samara) Next Senior Review in 2013 (bridge plus option contract planning has started). SST calibration issue is being remedied per Senior Review plans/recommendations:

Offloaded work from Davin who is busy on Maven, SP+ Performed calibrations and modeling at UCLA, cleanup software in place now (Drew Turner).

• THEMIS: a key player in the golden era of inner magnetosphere research Collaboration with RBSP (joint software with RBSP EFI/FGM, Key Params routines) Opportunity: Use White Sands 1 & Wallops (free) plus BGS (low cost) for 100% FS mode!!! Collaboration with TWINS, ERG, ORBITALS and ground (SD) teams under way

• ARTEMIS Lunar Orbit Insertions have occurred successfully on June 27 th –July 17th 2011 Planetary: LADEE conjunctions and crustal anomaly targets have been designed Instrument adjustments are under way

- Shadow despining software (local expert is Ferdinand Plaschke)- ESA/SST mode changes – will be magnetospheric only from now on

• Beyond 2014: MMS conjunctions with THEMIS and ARTEMIS Looking into orbit adjustments to line-up during MMS era – looking amazingly good!


ARTEMIS

THEMISPropagation of “bubble-like” jets fromreconnection site to near-Earth

Runov et al., 2009, 2010, 2011; Zhang et al., 2010; Li et al., 2011; Zhou et al., 2011 Curved flux tube Self-similar over global scales Low density Particle energization

~3 min 300 km/s

N V

V=velocity directionN=flux tube normal direction


ARTEMIS

THEMIS

(B) 8:18:54 UT

(C) 8:22:24 UT (D) 8:25:00 UT

(A) 8:14:54 UT

THEMIS All-sky imagers 2008-02-29

North-south arc

Poleward boundary

intensification

Arc contact and onset

Poleward expansion

Substorm macroscale interactions can beseen from the ground [Kepko/Nishimura/Lyons].

THEMIS GBOs linkReconnection andCurrent Disruption models

• Poleward boundary intensifications (enhanced magnetotail reconnection) supply fresh magnetotail lobe plasma to closed field lines.

• When the new plasma has low entropy, it reaches the near-Earth plasma sheet and triggers substorm expansion

• How are the dipolarization fronts interacting with each other and the inner magnetosphere?

• Interchange instability?• Deposition of energy?

Answers require both:• Kinetic exploration (FY10/11/12) and• Global exploration (FY13/14)

… of the equatorial magnetosphere inside of 12RE.


ARTEMIS

THEMISNon-substorm achievements: The originof pulsating aurora in the plasma sheet

Using coordinated satellite and ground-based all-sky observatories (GBOs) from the THEMIS mission, Nishimura et al. (Science, 2010) provide the first evidence that localized lower-band chorus waves observed at the equator, drive the pulsating aurora at a given pulsating patch in the ionosphere. The findings can also be used to constrain magnetic field models, an otherwise notoriously difficult task.

TH-ATH/GBO

THEMIS-A (P5) Magnetic Field

THEMIS-GBO ImagerAuroral and Chorus Intensity are correlated

THEMIS

ARTEMIS


Launch=2007-02-17

2007-03-23

2007-06-03

2007-07-15

2007-08-30

2007-12-04

XGSE

YGSE

TH-B

TH-C

TH-D

TH-E

TH-A

P1

P2

P3

P4

P5

First 10 months: Commissioning andCoast Phase Observations

THEMIS

ARTEMIS


Dayside 12008-08-08

XGSE

YGSE

First year THEMIS baseline orbit (FY08)

Dayside 22009-09-16

XGSE

YGSE

TH-B

TH-C

TH-D

TH-E

TH-A

P1

P2

P3

P4

P5 Second year baseline orbit (FY09)

Tail 12008-02-02

Tail 22009-02-18

Angelopoulos, 2008Space Sci. Rev.


ARTEMIS

THEMIS

THEMIS Extension (FY10,11,12)


ARTEMIS

THEMIS Electron beams accelerated byasymmetric wake potentialARTEMIS

ARTEMIS P1 electron spectra (a, b) and wake potential (c) inferred from them

Potential, V [Note: VC>VA>VB]

[Halekas et al., SSR, 2010]


ARTEMIS

THEMIS

ARTEMIS orbits

Note: P1 retrograde, and P2 prograde.

Relay conjunctions permit more monitoring time at periapsis, for periods of up to an hour.

Here P1 monitors the primary field while P2 measures the nightside induction field.

P1

P2


ARTEMIS

THEMIS ARTEMIS’s latest design satisfies LADEE conjunctions


ARTEMIS

THEMIS ARTEMIS’s design has optimized observations of crustal anomalies.


ARTEMIS

THEMISTHEMIS probe separations

2010-04-10 00:00:00

P3

P4

P5

X or -X

Z

FY 11/12

Tail or Dayside

Inner magnetosphere

2010-04-10 00:00:00

P3

P4

P5Z

FY 13/14

FY13: 4-8-12 hrs

FY14: 8-8-8 hrs

X or -X

P3


ARTEMIS

THEMIS

- Interaction of reconnection jet (or dipolarization front) with the inner

magnetosphere and its role in triggering substorms

P3

P3

P3

X

Z

P1Prime mission result: Reconnection starts first

FY 11/12 objective: Physics of reconnection-inner magnetosphere interaction

P2

intense waves

Jy ~ 100 nA/m2

Bz

(nT)

Bz

(nT)

Bz

(nT)

E(Hz)

elec

tron

s (f

)

30 keV

95 keV

P1P2P3

z

z

z

Jy

x

x

THEMIS Burst data

Runov et al. [2010]

P3P4

P5

Magnetotail from kinetic scales: FY11/12


ARTEMIS

THEMISThe Galaxy 15 knock-out:

AR-TH storm time conjunction

ART: P1

ART: P2THM:P3,4,5

ART: P1

ART: P2

THM: P3

THM: P4

THM: P5 Galaxy 15: damaged on Apr 5, 2010was only recovered on Apr 4, 2011

Connors et al., 2011 Ann. Geophys.

Connors et al., 2011 (Ann. Geophys.): GOES field over-dipolarized thanks to incoming flow bursts. How were particles accelerated? If only we had THEMIS in dispersed orbits, together RBSP there, we would now know!


ARTEMIS

THEMIS

- Cross-magnetotail width of reconnection and energetic particle injection regions

- Global evolution of energetic particle injections during substorms

3-6 RE

Magnetotail from global scales: FY13/14


ARTEMIS

THEMISMMS era (FY13/14): THEMIS observes RX drivers

2010-04-10 00:00:00

P3

P5

X or -X

Z

FY 14/15

MMS Phase2 or 1/3

P4

MMS

A tetrahedron within a tetrahedron

FY 15/16

P3P4

P5

MMS

P1

P2

Resonant orbits: alignments at solar max

X

Y


ARTEMIS

THEMISData Collection and Distribution

THEMIS GBOs

THEMIS/ARTEMIS PROBES

T-DASGround calibrationSoftware depositoryCDF and Cal. Files

MIRROREUROPE

MIRRORJAPAN

MIRRORTAIWAN

NASA(CDA, SSC)

Researcher

WWW

NOAA (GOES,SPIDR)

Indices(AE Index,Dst,Kp)

Ancillary GMAG (MACCS,Carisma,

Greenland, GIMA)

RBSP (EFI/FGM, others: Kp)

ERG

SuperDARN(GOES,SPIDR)


ARTEMIS

THEMIS

Backup slides

THEMIS

ARTEMIS


Data Processing and Community Support

• All data/plots available, calibrated 1 day after downlink (http://sprg.ssl.berkeley.edu)• Routine data distribution in 4 ways

– CDF downloads from SPDF, UCB, 4 mirror sites– HTTP and FTP socket connection through software (seemless)– Bundled downloads via UCB site (per instrument, spacecraft, product)– On-line at VMOs, and PDS (data is SPASE compatible).

• Free, powerful software distribution, on-line docs, tutorials– IDL-based, platform independent– Community demos biannually at GEM meetings + trainings on demand

• On-line Support ([email protected])• SVN configuraton-controlled: distributed, grass-roots effort• Community training sessions twice a year (GEM and AGU)


ARTEMIS

THEMISTHEMIS Software

themis/artemis, fall swt 1 sep. 14-16, 2011 artemis themis mission accomplishments, status li et al....

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